Deriving model-based Te-consistent chemical abundances in ionized gaseous nebulae

By E. P'erez-Montero. 2014

147 citations recorded by the source corpus.

The derivation of abundances in gaseous nebulae ionised by massive stars using optical collisionally excited emission lines is studied in this work comparing the direct or $T_e$ method with updated grids of photoionisation models covering a wide range of input conditions of O/H and N/O abundances and ionisation parameter. The abundances in a large sample of compiled objects with at least one auroral line are re-derived and later compared with the $\chi^2$ weighted-mean abundances from the models. The agreement between the abundances using the two methods both for O/H and N/O is excellent with no additional assumptions about the geometry or physics governing the HII regions. Although very inaccurate model-based O/H are obtained when no auroral lines are considered, this can be overcome assuming empirical laws between O/H, log $U$, and N/O to constrain the considered models. In this way, for 12+log(O/H) $>$ 8.0, a precision better than 0.1dex consistent with the direct method is attained. For very low-$Z$, models give higher O/H values and a high dispersion, possibly owing to the contamination of the low-excitation emission-lines. However, in this regime, the auroral lines are usually well-detected. The use of this procedure, in a publicly available script, HII-CHI-mistry}, leads to the derivation of abundances in faint/high redshift objects consistent with the direct method based on CELs.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/9158b9c00a44a47d87dcc383d6aa0c73ecfc99f5

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In Astronomy and Astrophysics

Citations in the corpus

De re metallica: the cosmic chemical evolution of galaxies (2018, background): “…an ionization correction for the unobserved ones, the total elemental abundance is derived (e.g., Aller, 1954; Dinerstein, 1990; Pilyugin & Thuan, 2005; Pilyugin et al., 2006b, 2009; Bresolin et al., 2009b; Pilyugin et al., 2010a; Perez-Martinez, 2014; Pérez-Montero, 2014; Pérez et al., 2016).”
THE MOSDEF SURVEY: ELECTRON DENSITY AND IONIZATION PARAMETER AT z ∼ 2.3 (2015, background): “…between M∗ and metallicity, known as the mass-metallicity relation (MZR; Lequeux et al. 1979; Tremonti et al. 2004; Kewley & Ellison 2008; Mannucci et al. 2010; Andrews & Martini 2013), and an anticorrelation between metallicity and ionization parameter (Pérez-Montero 2014; Sánchez et al. 2015).”
SDSS-IV MaNGA : the impact of diffuse ionized gas on emission-line ratios, interpretation of diagnostic diagrams and gas metallicity measurements (2016, background): “However, if one were to include a DIG model in IZI and other Bayesian codes to derive metallicities (e.g.,HII-CHI-mistry: Pérez-Montero 2014; BOND: Vale Asari et al 2016) , then they may be able to give accurate estimates of metallicity and ionization parameter even with contamination of DIG.”
SDSS IV MaNGA – metallicity and nitrogen abundance gradients in local galaxies (2017, background): “Despite recent advances (Dopita et al. 2013; Perez-Montero 2014; Blanc et al. 2015; Asari et al. 2016; Curti et al. 2017), reliably measuring the gas metallicity from strong emission lines ratios remains a difficult problem in observational astrophysics.”
An extreme [O III] emitter at z = 3.2: a low metallicity Lyman continuum source (2015, methodology): “We derive ionization parameter, Oxygen and Carbon abundances using a modified version of the HII-CHI-mistry code (Pérez-Montero 2014), adapted to provide metallicity, C/O and ionization parameter in a Te-consistent framework, based on the comparison of the observed UV and optical nebular lines…”
PyNeb: a new tool for analyzing emission lines - I. Code description and validation of results (2014, unknown): “…of papers (GarcíaRojas et al. 2012, 2013, 2014; Esteban et al. 2013, 2014; Kameswara Rao et al. 2013; Nicholls et al. 2013, 2014; Marino et al. 2013; Delgado-Inglada et al. 2014; Delgado-Inglada & Rodríguez 2014; Mesa-Delgado et al. 2014; Sankrit et al. 2014; Ho et al. 2014; Pérez-Montero 2014).”